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Aperture synthesis orsynthesis imaging is a type ofinterferometry that mixes signals from a collection oftelescopes to produce images having the sameangular resolution as an instrument the size of the entire collection.[1][2][3] At each separation and orientation, the lobe-pattern of the interferometer produces an output which is one component of theFourier transform of the spatial distribution of the brightness of the observed object. The image (or "map") of the source is produced from these measurements.Astronomical interferometers are commonly used for high-resolutionoptical,infrared,submillimetre andradio astronomy observations. For example, theEvent Horizon Telescope project derived the first image of a black hole using aperture synthesis.[4]
Aperture synthesis is possible only if both theamplitude and thephase of the incoming signal are measured by each telescope. For radio frequencies, this is possible by electronics, while for optical frequencies, the electromagnetic field cannot be measured directly and correlated in software, but must be propagated by sensitive optics and interfered optically. Accurate optical delay and atmospheric wavefront aberration correction are required, a very demanding technology that became possible only in the 1990s. This is why imaging with aperture synthesis has been used successfully in radio astronomy since the 1950s and in optical/infrared astronomy only since the turn of the millennium. Seeastronomical interferometer for more information.
In order to produce a high quality image, a large number of different separations between different telescopes is required (the projected separation between any two telescopes as seen from the radio source is called a baseline) – as many different baselines as possible are required in order to get a good quality image. The number of baselines (nb) for an array ofn telescopes is given bynb=(n2 − n)/2. (This is ornC2). For example, theVery Large Array has 27 telescopes giving 351 independent baselines at once, and can give high quality images.
In contrast to radio arrays, the largest optical arrays currently have only 6 telescopes, giving poorer image quality from the 15 baselines between the telescopes.
Most radio frequency aperture synthesis interferometers use the rotation of the Earth to increase the number of different baselines included in an observation (see diagram on right). Taking data at different times provides measurements with different telescope separations and angles without the need for additional telescopes or moving the telescopes manually, as the rotation of the Earth moves the telescopes to new baselines.
The use of Earth rotation was discussed in detail in the 1950 paperA preliminary survey of the radio stars in the Northern Hemisphere.[5] Some instruments use artificial rotation of the interferometer array instead of Earth rotation, such as inaperture masking interferometry.
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The concept of aperture synthesis was first formulated in 1946 by Australianradio astronomersRuby Payne-Scott andJoseph Pawsey. Working fromDover Heights inSydney, Payne-Scott carried out the earliestinterferometer observations in radio astronomy on 26 January 1946 using anAustralian Army radar as a radio telescope.[6]
Aperture synthesis imaging was later developed at radio wavelengths byMartin Ryle and coworkers from theRadio Astronomy Group atCambridge University. Martin Ryle andTony Hewish jointly received aNobel Prize for this and other contributions to the development of radio interferometry.
The radio astronomy group in Cambridge went on to found theMullard Radio Astronomy Observatory near Cambridge in the 1950s. During the late 1960s and early 1970s, as computers (such as theTitan) became capable of handling the computationally intensive Fourier transform inversions required, they used aperture synthesis to create a 'One-Mile' and later a '5 km' effective aperture using theOne-Mile andRyle telescopes, respectively.
The technique was subsequently further developed invery-long-baseline interferometry to obtain baselines of thousands of kilometers and even inoptical telescopes. The termaperture synthesis can also refer to a type ofradar system known assynthetic aperture radar, but this is technically unrelated to the radio astronomy method and developed independently.
Originally it was thought necessary to make measurements at essentially every baseline length and orientation out to some maximum: such afully sampled Fourier transform formally contains the information exactly equivalent to the image from a conventional telescope with an aperture diameter equal to the maximum baseline, hence the nameaperture synthesis.
It was rapidly discovered that in many cases, useful images could be made with a relatively sparse and irregular set of baselines, especially with the help of non-lineardeconvolution algorithms such as themaximum entropy method. The alternative namesynthesis imaging acknowledges the shift in emphasis from trying to synthesize the complete aperture (allowing image reconstruction by Fourier transform) to trying to synthesize the image from whatever data is available, using powerful but computationally expensive algorithms.
To avoid this computational bottleneck, telescopes such as theDSA-2000 use a large number (in this case 2000) randomly distributed antennas to nearly fully sample theuv plane. This gives apoint spread function that allows much simpler reconstruction, so images can be computed as the data comes off the telescope. This is referred to as aradio camera.
Note that aperture synthesis is technically and historically independent ofsynthetic aperture radar, which is aDoppler technique, originally developed in the early 1950s byCarl A. Wiley. The operating principles are unrelated.[7]
